Mu Ceti

{{Starbox begin

| name = μ Ceti

}}

{{Starbox image

| image=

{{Location mark

|image=Cetus constellation map.svg|alt=|float=center|width=280

|label=|position=right

|mark=Red circle.svg|mark_width=10|mark_link=μ Cei

|x=206|y=86

}}

|caption=Location of μ Ceti (circled)

}}

{{Starbox observe

| epoch=J2000.0

| constell=Cetus

| ra= {{RA|02|44|56.53735}}

| dec= {{DEC|+10|06|50.9217}}

| appmag_v=+4.27 (4.30 + 7.80)

}}

{{Starbox character

| type = Main sequence

| class =A9IIIp + K0.5V

| variable = Gamma Doradus

}}

{{Starbox astrometry

| radial_v = {{val|+29.53|0.28}}

| prop_mo_ra = {{val|+278.641}}

| prop_mo_dec = {{val|-41.222}}

| pm_footnote =

| parallax = 37.5924

| p_error = 0.2440

| parallax_footnote =

| dist_ly =

| dist_pc =

| absmag_v = +2.17

}}

{{Starbox detail

| source =

| component1 = A

| mass = {{val|1.66|0.04}}

| radius = {{val|2.07|0.11}}

| luminosity = {{val|10.1|0.4}}

| temperature = {{Val|7380|180|fmt=commas}}

| metal = {{M/H|{{val|0.06|0.03}}}}

| gravity = {{val|3.92|0.23}}

| rotational_velocity = {{Val|45.1|2.3}}

| age_gyr = {{val|1.20|0.18|0.16}}

| component2 = B

| mass2 = {{val|0.80|0.10}}

| radius2 = {{val|0.80|0.15}}

| temperature2 = 5,250

}}

{{Starbox orbit

| primary = A

| name = B

| reference =

| period = {{val|33.62|0.03}}

| axis = {{val|0.5259|0.0026}}

| eccentricity = {{val|0.9219|0.0006}}

| inclination = {{val|95.5|0.4}}

| node = {{val|59.18|0.06}}

| periarg = {{val|78.26|0.01}}

| periastron = {{val|2019.33|fmt=none}} yr

}}

{{Starbox catalog

| names=87 Ceti, HD 17094, HIP 12828, HR 813, SAO 110723, BD+09°359

}}

{{Starbox reference

| Simbad=87+Cet

}}

Mu Ceti (μ Ceti) is a binary star in the constellation Cetus, the whale, close to Pisces. The combined apparent magnitude of the system is +4.27, making it visible as a faint star from skies with low or no luminous pollution. Based upon parallax measurements taken by the Gaia spacecraft, it is located 87 light-years away.

The location of Mu Ceti next to the ecliptic make it succeptible to lunar occultations.

Nomenclature

Mu Ceti is the system's Bayer designation. It has no official proper name.

In Chinese, {{lang|zh|天囷}} ({{lang|zh-Latn|Tiān Qūn}}), meaning Circular Celestial Granary, refers to an asterism consisting of α Ceti, κ¹ Ceti, λ Ceti, μ Ceti, ξ¹ Ceti, ξ² Ceti, ν Ceti, γ Ceti, δ Ceti, 75 Ceti, 70 Ceti, 63 Ceti and 66 Ceti. Consequently, the Chinese name for Mu Ceti itself is "the Fourth Star of Circular Celestial Granary".{{in lang|zh}} [http://aeea.nmns.edu.tw/2006/0607/ap060711.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日] {{Webarchive|url=https://web.archive.org/web/20120204114123/http://aeea.nmns.edu.tw/2006/0607/ap060711.html |date=2012-02-04 }}

Characteristics

File:MuCetLightCurve.png for Mu Ceti plotted from TESS data]]

Mu Ceti is a spectroscopic binary. These systems have binarity inferred from variations in their spectral lines, which shift from redder to bluer (gravitational redshift) across the orbit. It has also been resolved by speckle interferometry. The energy output is dominated by the main star, which is 25 times brighter than the companion.{{efn|name=magnitudes}} They share a highly eccentric orbit, are viewed orbiting nearly edge-on, and take 34 years to complete an orbit.

The main component (apparent magnitude 4.30) has an spectral class A9IIIp, suggesting it is a late-type giant star and is chemically peculiar. Its physical properties, however, do not support this evolutionary stage and the peculiar class, Mu Ceti is instead in the late main sequence, about to become a subgiant. This star is 67% more massive than the Sun and two times larger. Its effective temperature is {{val|7380|u=Kelvin}}, giving it the white hue typical of late A/early F stars. It has been suspected to be a δ Scuti variable, and found to be of constant brightness by some studies, but a more recent analysis with the Transiting Exoplanet Survey Satellite confirm this star is a Gamma Doradus variable.

The secondary (apparent magnitude 7.80) is a K0.5V star, indicating it is a dwarf star cooler than the Sun. Mu Ceti B has an effective temperature of {{val|5250|fmt=commas|ul=K}} and has a mass and radius measuring 80% solar units. Its effective temperature give it an orange hue typical of K-type stars.

Three companions were all discovered during occultations of Mu Ceti by the Moon. An orbit was derived for the brightest with a period of 1,202 days. Later studies have failed to find any evidence of these companions.

Notes

{{Notelist|notes=

{{Efn|name=magnitudes|1=Inferred from magnitude differences. The equation is: $\sqrt[5]{100}$ ^$(7.8-4.3)$ ≈ 25.}}

}}

References

{{reflist|refs=

{{cite web

| title=MAST: Barbara A. Mikulski Archive for Space Telescopes

| url=https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html

| publisher=Space Telescope Science Institute |access-date=14 September 2024}}

{{Cite journal |last1=Dyachenko |first1=V. V. |last2=Yakunin |first2=I. A. |last3=Bayazitov |first3=R. M. |last4=Grigoriev |first4=S. A. |last5=Ryabchikova |first5=T. A. |last6=Pakhomov |first6=Yu. V. |last7=Semenko |first7=E. A. |last8=Beskakotov |first8=A. S. |last9=Mitrofanova |first9=A. A. |last10=Maksimov |first10=A. F. |last11=Balega |first11=Yu. Yu. |date=2024-09-01 |title=Study of the μ Cet Binary with Speckle Interferometric, Photometric, and Spectroscopic Techniques |journal=Astrophysical Bulletin |volume=79 |issue=3 |pages=445–463 |doi=10.1134/S1990341324600698 |arxiv=2409.15063 |bibcode=2024AstBu..79..445D}}

{{Cite journal |last1=Dyachenko |first1=V. |last2=Richichi |first2=A. |last3=Balega |first3=Yu |last4=Beskakotov |first4=A. |last5=Maksimov |first5=A. |last6=Mitrofanova |first6=A. |last7=Rastegaev |first7=D. |date=2018-08-01 |title=Lunar occultation observations at the SAO RAS 6-m telescope |bibcode=2018MNRAS.478.5683D |journal=Monthly Notices of the Royal Astronomical Society |volume=478 |issue=4 |pages=5683–5688 |doi=10.1093/mnras/sty1427 |doi-access=free |issn=0035-8711}}

{{cite journal|bibcode=1971A&A....11...79H|title=Short period variable stars. V. Delta Scuti-type stars in the Geneva system|journal=Astronomy and Astrophysics|volume=11|pages=79|last1=Hauck|first1=B|year=1971}}

{{cite journal|bibcode=1969ApJS...19...79B|title=Short-Period Variability of b, a, and F Stars. III. A Survey of Delta Scuti Variable Stars|journal=Astrophysical Journal Supplement|volume=19|pages=79|last1=Breger|first1=Michel|year=1969|doi=10.1086/190199}}

{{cite web |title=The Colour of Stars |date=December 21, 2004 |work=Australia Telescope, Outreach and Education |publisher=Commonwealth Scientific and Industrial Research Organisation |url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |access-date=2012-01-16 |url-status=dead |archive-url=https://web.archive.org/web/20120318151427/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |archive-date=2012-03-18 }}

{{cite journal|bibcode=2016ApJS..227....4H|arxiv=1609.05254|title=Surveying the Bright Stars by Optical Interferometry. I. A Search for Multiplicity among Stars of Spectral Types F-K|journal=The Astrophysical Journal Supplement Series|volume=227|pages=4|last1=Hutter|first1=D. J|last2=Zavala|first2=R. T|last3=Tycner|first3=C|last4=Benson|first4=J. A|last5=Hummel|first5=C. A|last6=Sanborn|first6=J|last7=Franz|first7=O. G|last8=Johnston|first8=K. J|year=2016|issue=1|doi=10.3847/0067-0049/227/1/4|s2cid=118803592 |doi-access=free }}

{{cite journal |last1=McDonald |first1=I. |last2=Zijlstra |first2=A. A. |last3=Watson |first3=R. A. |date=2017-10-01 |title=Fundamental parameters and infrared excesses of Tycho-Gaia stars |journal=Monthly Notices of the Royal Astronomical Society |volume=471 |issue=1 |pages=770–791 |doi=10.1093/mnras/stx1433 |doi-access=free |issn=0035-8711|arxiv=1706.02208 |bibcode=2017MNRAS.471..770M }} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/MNRAS/471/770&RAJ2000=041.235593 Mu Ceti's database entry] at VizieR.

{{cite journal | last1=Reiners | first1=Ansgar | title=Rotation- and temperature-dependence of stellar latitudinal differential rotation | journal=Astronomy and Astrophysics | volume=446 | issue=1 |date=January 2006 | pages=267–277 | doi=10.1051/0004-6361:20053911 | bibcode=2006A&A...446..267R |arxiv = astro-ph/0509399 | s2cid=8642707 }}

{{cite web|url=http://stars.astro.illinois.edu/sow/mucet.html|title=Mu Ceti|author=Jim Kaler|date=Dec 21, 2007}}

{{cite journal|bibcode= 2003AJ....126.2048G |title= Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I |journal= The Astronomical Journal |volume= 126 |issue= 4 |pages= 2048 |last1= Gray |first1= R. O |last2= Corbally |first2= C. J |last3= Garrison |first3= R. F |last4= McFadden |first4= M. T |last5= Robinson |first5= P. E |year= 2003 |doi= 10.1086/378365 |arxiv= astro-ph/0308182 |s2cid= 119417105 }}

{{cite journal|bibcode=2001A&A...367..297A|title=Research Note Hipparcos photometry: The least variable stars|journal=Astronomy and Astrophysics|volume=367|pages=297–298|last1=Adelman|first1=S. J|year=2001|doi=10.1051/0004-6361:20000567|doi-access=free}}

{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}

{{cite journal

| title=Identification List of Spectroscopic and Eclipsing Binaries Subject to Occultations by the Moon

| last=Herr | first=Richard B.

| journal=Publications of the Astronomical Society of the Pacific

| volume=81 | issue=479 | page=105 | date=April 1969

| doi=10.1086/128748 | bibcode=1969PASP...81..105H }}

}}

Category:Cetus

Ceti, Mu

Category:F-type main-sequence stars

Ceti, 87

012828